caa a22 4500 445346361 CHVBK 20180317142830.0 cr unu---uuuuu 170323e20110801xx s 000 0 eng 10.1007/s11207-011-9811-9 doi (NATIONALLICENCE)springer-10.1007/s11207-011-9811-9 Tracking a Ulysses High-latitude ICME Event Back to Its Solar Origins [Elektronische Daten] [C. Dumitrache, N. Popescu, A. Oncica] High-latitude interplanetary mass ejections (ICMEs) observed beyond 1 AU are not studied very often. They are useful for improving our understanding of the 3D heliosphere. As there are only few such events registered by the Ulysses spacecraft, the task of detecting their solar counterparts is a challenge, especially during high solar activity periods, because there are dozens coronal mass ejections (CMEs) registered by SOHO that might be chosen as candidates. We analyzed a high-latitude ICME registered by the Ulysses spacecraft on 18 January 2002. Our investigation focused on the correlation between various plasma parameters that allow the identification to be made of the ICME and its components such as the forward shock, the magnetic cloud and the reverse shock. Using a linear approach and a graphical method we have been able to track the ICME event back to the Sun and to compute the day of the occurrence of the solar CME. In order to decide among several CME candidates which one is the right solar counterpart of our event, we have performed a follow-up computation of these CMEs from the Sun to Ulysses, by using two different speed formulas. First, the computation was simply based on the initial CME velocity, while the other was based on the ICME velocity estimated from the CME initial speed (Lindsay et al. 1999). Differences of hours have been obtained between the arrival time predicted in these two ways, but the second one gave the best results. Both methods indicated the same two CMEs as the solar counterparts. We have found the solar source of these CMEs as being a huge polar filament that erupted in several steps. This ICME event displayed a double magnetic cloud configuration. Aminimum variance analysis helped us to detect the smooth rotation of the clouds and their helicity. Both magnetic clouds show the same helicity as the filament that erupted and released them. Acylinder-shape model of both clouds gives the same helicity sign. Springer Science+Business Media B.V., 2011 Coronal mass ejections nationallicence Interplanetary coronal mass ejections nationallicence Magnetic clouds nationallicence Prominences nationallicence Dumitrache C. Astronomical Institute of Romanian Academy, 040557, Bucharest, Romania aut Popescu N. Astronomical Institute of Romanian Academy, 040557, Bucharest, Romania aut Oncica A. Astronomical Institute of Romanian Academy, 040557, Bucharest, Romania aut Solar Physics Springer Netherlands 272/1(2011-08-01), 137-157 0038-0938 272:1<137 2011 272 11207 https://doi.org/10.1007/s11207-011-9811-9 text/html Onlinezugriff via DOI 1 research-article jats NATIONALLICENCE 856 40 https://doi.org/10.1007/s11207-011-9811-9 text/html Onlinezugriff via DOI NATIONALLICENCE 700 1- Dumitrache C. Astronomical Institute of Romanian Academy, 040557, Bucharest, Romania aut NATIONALLICENCE 700 1- Popescu N. Astronomical Institute of Romanian Academy, 040557, Bucharest, Romania aut NATIONALLICENCE 700 1- Oncica A. Astronomical Institute of Romanian Academy, 040557, Bucharest, Romania aut NATIONALLICENCE 773 0- Solar Physics Springer Netherlands 272/1(2011-08-01), 137-157 0038-0938 272:1<137 2011 272 11207 Metadata rights reserved Springer special CC-BY-NC licence nationallicence BK010053 XK010053 XK010000 NATIONALLICENCE NATIONALLICENCE NL-springer